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Smith, Lance A.; Jackson, Michael; Al-Barghouthy, Ghassan; Jenner, Peter

doi:10.1007/s007020200009

Cited by 161 publications

(194 citation statements)

References 49 publications

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“…The galaxies were selected from multi-colour SDSS imaging (Fukugita et al 1996;Gunn et al 1998;Smith et al 2002;Gunn et al 2006;Doi et al 2010) focussing on the redshift range of 0.15 z 0.70. The galaxy survey used two primary target algorithms, selecting samples called LOWZ, with 361 762 galaxies in the final data release DR12 (Alam et al 2015a) between 0.15 z 0.43 and CMASS, with 777 202 galaxies in DR12 between 0.43 z 0.70.…”

Section: The Sdss III Boss Datamentioning

confidence: 99%

The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: RSD measurement from the LOS-dependent power spectrum of DR12 BOSS galaxies

Gil-Marín¹,

Percival²,

Brownstein³

et al. 2016

Mon. Not. R. Astron. Soc.

169

247

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We measure and analyse the clustering of the Baryon Oscillation Spectroscopic Survey (BOSS) relative to the line-of-sight (LOS), for LOWZ and CMASS galaxy samples drawn from the final Data Release 12 (DR12). The LOWZ sample contains 361 762 galaxies with an effective redshift of z lowz = 0.32, and the CMASS sample 777 202 galaxies with an effective redshift of z cmass = 0.57. From the power spectrum monopole and quadrupole moments around the LOS, we measure the growth of structure parameter f times the amplitude of dark matter density fluctuations σ 8 by modeling the Redshift-Space Distortion signal. When the geometrical Alcock-Paczynski effect is also constrained from the same data, we find joint constraints on f σ 8 , the product of the Hubble constant and the comoving sound horizon at the baryon drag epoch H(z)r s (z d ), and the angular distance parameter divided by the sound horizon D A (z)/r s (z d ). We find f (z lowz )σ 8 (z lowz ) = 0.394 ± 0.062, D A (z lowz )/r s (z d ) = 6.35 ± 0.19, H(z lowz )r s (z d ) = (11.41 ± 0.56) 10 3 kms −1 for the LOWZ sample, and f (z cmass )σ 8 (z cmass ) = 0.444 ± 0.038, D A (z cmass )/r s (z d ) = 9.42 ± 0.15, H(z cmass )r s (z d ) = (13.92 ± 0.44) 10 3 kms −1 for the CMASS sample. We find general agreement with previous BOSS DR11 measurements. Assuming the Hubble parameter and angular distance parameter are fixed at fiducial ΛCDM values, we find f (z lowz )σ 8 (z lowz ) = 0.485 ± 0.044 and f (z cmass )σ 8 (z cmass ) = 0.436 ± 0.022 for the LOWZ and CMASS samples, respectively.

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Section: The Sdss III Boss Datamentioning

confidence: 99%

The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: RSD measurement from the LOS-dependent power spectrum of DR12 BOSS galaxies

Gil-Marín¹,

Percival²,

Brownstein³

et al. 2016

Mon. Not. R. Astron. Soc.

169

247

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“…The basis of the photometric calibration of the SDSS is defined by the 158 primary standards measured by the USNO 40-inches telescope (Smith et al 2002), which however has filters with different effective wavelengths than those of the SDSS 2.5m survey telescope 10 . The latter defines the unprimed ugriz system for which photometry has been published from SDSS DR1 onward, and for which we provide synthetic colours in this work.…”

Section: Sloan Digital Sky Survey Ugrizmentioning

confidence: 99%

Synthetic stellar photometry – I. General considerations and new transformations for broad-band systems

Casagrande¹,

VandenBerg²

2014

Monthly Notices of the Royal Astronomical Society

257

321

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After a pedagogical introduction to the main concepts of synthetic photometry, colours and bolometric corrections in the Johnson-Cousins, 2MASS, and HST-ACS/WFC3 photometric systems are generated from MARCS synthetic fluxes for various [Fe/H] and [α/Fe] combinations, and virtually any value of E(B − V) 0.7. The successes and failures of model fluxes in reproducing the observed magnitudes are highlighted. Overall, extant synthetic fluxes predict quite realistic broad-band colours and bolometric corrections, especially at optical and longer wavelengths: further improvements of the predictions for the blue and ultraviolet spectral regions await the use of hydrodynamic models where the microturbulent velocity is not treated as a free parameter. We show how the morphology of the colour-magnitude diagram (CMD) changes for different values of [Fe/H] and [α/Fe]; in particular,how suitable colour combinations can easily discriminate between red giant branch and lower main sequence populations with different [α/Fe], due to the concomitant loops and swings in the CMD. We also provide computer programs to produce tables of synthetic bolometric corrections as well as routines to interpolate in them. These colour-T eff -metallicity relations may be used to convert isochrones for different chemical compositions to various bandpasses assuming observed reddening values, thus bypassing the standard assumption of a constant colour excess for stars of different spectral type. We also show how such an assumption can lead to significant systematic errors. The MARCS transformations presented in this study promise to provide important constraints on our understanding of the multiple stellar populations found in globular clusters (e.g., the colours of lower main sequence stars are predicted to depend strongly on [α/Fe]) and of those located towards/in the Galactic bulge.

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“…degrees of sky obtained using a 2.5 m telescope at Apache Point Observatory (York et al 2000;Gunn et al 2006;Alam et al 2015). A series of publications outlines the technical details of SDSS instrumentation (Fukugita et al 1996;Smith et al 2002;Doi et al 2010;Smee et al 2013) and the data processing pipelines (Lupton et al 2001;Pier et al 2003;Padmanabhan et al 2008;Bolton et al 2012;Weaver et al 2015). We perform our analysis on the CMASS sample of BOSS galaxies, which is defined via colour and magnitude cuts as in Eisenstein et al (2011), Dawson et al (2013), and Reid et al (2015).…”

Section: Datamentioning

confidence: 99%

Quantifying the colour-dependent stochasticity of large-scale structure

Patej

Eisenstein

2016

Mon. Not. R. Astron. Soc.

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We address the question of whether massive red and blue galaxies trace the same largescale structure at z ∼ 0.6 using the CMASS sample of galaxies from Data Release 12 of the Sloan Digital Sky Survey III. After splitting the catalog into subsamples of red and blue galaxies using a simple colour cut, we measure the clustering of both subsamples and construct the correlation coefficient, r, using two statistics. The correlation coefficient quantifies the stochasticity between the two subsamples, which we examine over intermediate scales (20 R 100 h −1 Mpc). We find that on these intermediate scales, the correlation coefficient is consistent with 1; in particular, we find r > 0.95 taking into account both statistics and r > 0.974 using the favored statistic.

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Untitled

Cited by 161 publications

References 49 publications

The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: RSD measurement from the LOS-dependent power spectrum of DR12 BOSS galaxies

The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: RSD measurement from the LOS-dependent power spectrum of DR12 BOSS galaxies

Synthetic stellar photometry – I. General considerations and new transformations for broad-band systems

Quantifying the colour-dependent stochasticity of large-scale structure

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